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<ri:Resource created="2011-05-13T14:39:59Z" status="active" updated="2025-06-13T15:25:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>MgI and sTiO index definitions</title><shortName>J/MNRAS/396/1895</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/396/1895</identifier><altIdentifier>doi:10.26093/cds/vizier.73961895</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Cenarro A.J.</name></creator><creator><name>Cardiel N.</name></creator><creator><name>Vazdekis A.</name></creator><creator><name>Gorgas J.</name></creator><date role="Updated">2024-07-08T20:15:58Z</date><date role="Created">2011-05-13T14:39:59Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>globular-star-clusters</subject><subject>spectroscopy</subject><description>Using the near-infrared spectral stellar library of Cenarro et al. (J/MNRAS/326/959), the behaviour of the MgI line at 8807{AA} and nearby TiO bands is analyzed in terms of the effective temperature, surface gravity and metallicity of the library stars. New spectroscopic indices for both spectral features - namely MgI and sTiO - are defined, and their sensitivities to different signal-to-noise ratios, spectral resolutions, flux calibrations and sky emission-line residuals are characterized. The two new indices exhibit interesting properties. In particular, MgI is a good indicator of the Mg abundance, whereas sTiO is a powerful dwarf-to-giant discriminator for cold spectral types. Empirical fitting polynomials that reproduce the strength of the new indices as a function of the stellar atmospheric parameters are computed, and a fortran routine with the fitting function predictions is made available. A thorough study of several error sources, non-solar [Mg/Fe] ratios and their influence on the fitting function residuals is also presented. From this analysis, an [Mg/Fe] underabundance of ~-0.04 is derived for the Galactic open cluster M67.</description><source format="bibcode">2009MNRAS.396.1895C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/396/1895</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/326/959">J/MNRAS/326/959 : Near-IR Ca triplet empirical calibration (Cenarro+ 2001)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Seq</name><description>Sequential number</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>SpType</name><description>MK spectral type</description><ucd>src.spType</ucd><dataType xsi:type="vs:VOTableType" arraysize="13*">char</dataType></column><column><name>MgI</name><description>MgI index measurement</description><unit>0.1nm</unit><ucd>spect.index</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_MgI</name><description>rms uncertainty on MgI (2)</description><unit>0.1nm</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>dMgI</name><description>? Fitting function residual for MgI</description><unit>0.1nm</unit><ucd>stat.fit.residual</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>sTiO</name><description>sTiO index measurement</description><unit>0.1nm</unit><ucd>spect.index</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_sTiO</name><description>rms uncertainty on sTiO (2)</description><unit>0.1nm</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>dsTiO</name><description>? Fitting function residual for IsTiO</description><unit>0.1nm</unit><ucd>stat.fit.residual</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>[Mg/Fe]</name><description>? [Mg/Fe] abundances (when available)</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>r_[Mg/Fe]</name><description>? 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